T\(_{\rm {He}}\)  also depends on the total mass of the white dwarf merger [1]}; however, the exact dependence has not been studied extensively. The [2]} estimates mentioned above assumed M\(_{\rm {tot}} \approx 0.9\)  M\(_{\odot }\) . Without including nucleosynthetic energy, [1]} found that a M\(_{\rm {tot}} = 0.7\)  M\(_{\odot }\) , \(q=0.5\)  merger has T\(_{\rm {He}}<2\times 10^{8}\)  K – lower than the estimate of \(3\times 10^{8}\)  K for the 0.9 M\(_{\odot }\) , \(q=0.5\)  merger. This suggests that lower mass mergers have lower T\(_{\rm {He}}\)  than higher mass mergers. Adding nucleosynthetic energy can increase T\(_{\rm {He}}\)  for the 0.7 M\(_{\odot }\)  merger to the dLHdC range (\(2.5-3.5\times 10^8\)  K) and the 0.9 M\(_{\odot }\)  merger outside this range. dLHdC stars would then be consistent with arising from lower mass mergers than RCB stars. This would be consistent with the observation in Tisserand et al. (2021) that the population of dLHdC stars has lower luminosities than RCB stars, which they interpret as a consequence of dLHdC stars originating from lower mass mergers than RCB stars.
